Type-I migration, the tidal migration of embedded protoplanets, poses
a significant challenge to Jovian planet formation while at the same
time providing a mechanism to form short-period, low-mass planets.
Recent theoretical work on type I migration underscores the importance
of the protoplanetary disk structure, including the thermal
properties, on the rates and even direction of migration. In this
talk I will discuss the implications of these new type I migration
rates on the formation of planets and planetary systems. In
particular, I compare the migration of planets in standard "alpha"
disk models to that expected in disks which evolve due to turbulence
driven by the magneto-rotational instability (MRI).